Lots to Do!
In the stretch of the moon cycle where I can get some practice and assembly done, I have these goals before the outing. Nearly all have to be done under the sky where I can test by using stars. Even with the moon waxing, there are some bright stars to use for all exercises.
1. Align the DSLR with the SV4 so that the flattener is optimally placed.
I have been using the SSF6 flattner for many years. It's only been in the last year that I've become aware of a standard procedure for testing flatness and star size. This method requires taking sample pictures and passing them through CCD Inspector for flatness and tilt. Each time I'll need to tweak the alignment a bit. It's down to shimming the tube and rings to ensure that the sensor is aligned as much as possible. Luckily, the alignment is getting closer and closer.
Interestingly, I backed out of the tilting device I'd made earlier. It did provide some tilt control but it placed a lot of horizontal strain on the focuser and camera mount. The flatness of the setup left a lot to be desired.
As an important reference, I have gone back to my earlier subs and checked and I see that the flatness is all over the place. Either the focuser wobbled or the way that the system flexed was giving horrible results. The lesson here is that with all the work I've done, this year should give me great results.
Not only am I concerned about the alignment with the optical center of the scope with the flattner, I am also trying to optimize the distance from the flattener to the sensor. I've been using a 1 mm spacer ring to give the optimal distance as 57 mm. Now that I'm doing even more testing, I'll get into it and check again. It's possible that less or even more will need to be added. I may go so far as adding a 7 mm segment.
2. Fine tune the polar alignment process.
To this end, I've started using PHD2. I had also been using the V method of imaging. While it's a great tool, it can be slow. I tried the PHD2 polar alignment method and it works very well.
The trick is to watch the trend lines while having DEC guiding off. DEC still must be calibrated for this to work. Once it's off and the scope is pointing to the right part of the sky, the graph trend lines will float to show how any cumulative drift is appearing.
Last night, AZ was pretty easy. ALT was more difficult mainly because it was such a hairtrigger adjustment. Approaching the perfect spot was hard with using just hands on the adjustment knob. I will try using a wrench on it -- maybe even something as simple as putting a pipe clamp on the outside of it will give a purchase for fingers. A better lever arm would be nice.
With this polar alignment done, I can estimate that the effort got the scope pointed very well - about 1 arc minute.
3. Tweak Maxim settings for best guiding.
As a nice bonus to the work I've been doing with fixing the flattener, I was able to remove much of the stress on the guide scope. This has made the guide stars nice and round again.
I think that I can safely say that Maxim is properly set for now.
4. Understand the difference of noise floor and sky glow with my camera setup.
|Suburban density (1200 seconds at 100 ISO)|
|Montebello density (1200 seconds at 100 ISO)|
|Calstar density (600 seconds at 400 ISO)|
In practice, there is no real value to increasing a sub length once the sky glow exceeds the noise floor. The noise floor for the K10D is defined by dark current and readout noise. This readout noise is about .7 in the Bias frames. In the full testing that I've done, the readout noise is about 2-3 ADU at 100 ISO. Dark current is based on the temperature. The full testing I've done says that the dark current at 20C is .077 e/pixel/sec for the green channel.
If I understand that dark current properly, then Bias is about 3 ADU, plus a dark current of 638 e (.07667 / 10M pixels / 1200 seconds) or 37 ADU, to give about 40 ADU as a total noise floor at 20 C.
The full well capacity is suggested to be 71399 e, so dividing this by the gain gives about 4199 ADU, which is near enough to the 12 bit limit of 4095 ADU. Subtract the noise floor and we're left with 4095 - 40 ADU = 4055 ADU headroom for skyglow.
The challenge is that skyglow varies. In the city, skyglow can be reached quickly. For example, my recent exposures of the Pacman nebula showed average values of 119 ADU in the gaps between stars. That's not bad, considering what we're assuming is the noise floor. At Montebello OSP, I was seeing background numbers of 37 ADU. That means that I could expose at MB for 3 times longer to reach the same density as I do at home or vice-versa.
The question becomes, are my 1200 second exposures at MB long enough? Strangely, I can do this test from at home, using my light polluted skies. The advantage here is that the light pollution registers faster and thus I can do the test quicker.
Here's what needs to be done: create a series of exposures that increment in duration. Then I look at them later and see at what point the bias signal disappears and then the dark noise profile starts to show. Increasing further, the skyglow should begin to register.
I've already done exposures of 10 seconds, 15 seconds, 120 seconds, 180 seconds. I also have exposures of 1200 seconds. What I miss are exposures of 600 seconds and 300 seconds. Once I have these set, I can compare. What I'm hoping to see is a point where the background skyglow shows up.
Once the skyglow gets bigger than the noise floor, then the subs are just loosing headroom. The annoying factor is that when this happens, whatever faint objects are also lost in the noise. It takes many sub exposures to build up the signal to noise ratio to compare with a dark sky site.
What do I expect? I think that I will see that I could do exposures that are 1/2 to 1/3 as long at home to reach the same level of density as I've seen at MB. What I would do at this point is see if there's enough signal to be worthwhile. Does an exposure of 300 to 400 seconds have enough signal?
This would mean having to make a whole new library of darks at different lengths.
As a followup question, if MB gives densities of 37 ADU for 1200 seconds at 100 ISO what does CALSTAR give? Looking at one of my subs (600 seconds at 400 ISO) I see background values of 65 ADU. Doing the simple math of comparing duration and ISO, an expected density of 32 ADU for 1200 seconds at 100 ISO should be what I'd expect at CALSTAR.
Will that be enough to get above the noise floor? Yes, just barely. It also says that on a good night, MB skies are nearly as dark as CALSTAR.
5. Set up and trial the GM8 for use as a wide field platform for film.
The GM8 currently has a Gemini 1 on it. I've never learned how to use the Gemini 1 in practice, so this would be a big step for my understanding. Luckily, Marek and a few others are using this version, so I can ask for help. The real challenges I see are: learning to do alignments on both sides of the meridian so that a flip can be done with some accuracy, and getting good guiding from the Nexstar device. I feel fairly confident about the first point, not so confident about the second.